The evolutionary sequence of planetary nebulae

Dopita, Michael A.; Meatheringham, S. J.

doi:10.1086/168900

Cited by 81 publications

(109 citation statements)

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“…The wisp is considerably fainter in the blue, Aller (1956). b Dopita & Meatheringham (1990). being barely visible at the plate limit on the SERC EJ survey.…”

Section: Aao/ukst Hα Survey Imagementioning

confidence: 96%

“…The spectrum shows very strong similarity to the bright eastern section of Sh 2-216 (Fesen, Blair, & Gull 1981), though the [Nii] emission is somewhat stronger; this may be an abundance effect. A decimal excitation class of 0.6 was calculated according to the scheme of Dopita & Meatheringham (1990). Both indices indicate a nebula of low excitation, as expected for a highly evolved PN of large intrinsic diameter surrounding a faint evolved central star on the white dwarf cooling track.…”

Section: Other Nebular Parametersmentioning

confidence: 99%

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PFP 1: A Large Planetary Nebula Caught in the First Stages of ISM Interaction

Pierce

Frew

Parker

et al. 2004

Publ. – Astron. Soc. Aust

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This paper presents (Hα + [Nii]) imaging and spectroscopy of a previously unknown, highly evolved planetary nebula of low excitation which is in the first stages of an interaction with the interstellar medium (ISM). It was discovered serendipitously from AAO/UKST Hα Survey images as part of a project to exploit the survey data and has evaded detection by previous surveys due to its very low surface brightness. It is a remarkable hollow-sphere planetary nebula, some 19 across, making it one of the largest examples of its type. We estimate a radius of 1.5 pc and a distance of 550 pc as derived from a new Hα surface brightnessradius relation. PFP 1 has near-perfect circular symmetry, broken only at the north-western edge which is coupled with significantly increased (Hα + [Nii]) intensity, both of which provide evidence for an interaction with the ISM. We find a near solar composition for this object with possibly enhanced He and N abundances. A blue central star candidate has been identified from the SuperCosmos Sky Survey data.

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“…The wisp is considerably fainter in the blue, Aller (1956). b Dopita & Meatheringham (1990). being barely visible at the plate limit on the SERC EJ survey.…”

Section: Aao/ukst Hα Survey Imagementioning

confidence: 96%

Section: Other Nebular Parametersmentioning

confidence: 99%

PFP 1: A Large Planetary Nebula Caught in the First Stages of ISM Interaction

Pierce

Frew

Parker

et al. 2004

Publ. – Astron. Soc. Aust

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“…Equations (5) constitute a purely empirical definition of the nebular excitation state in close resemblance to the original Morgan (1984) classification scheme (cf. Dopita & Meatheringham 1990). Although the low excitation branch, E < 5, depends directly on the oxygen abundance, Eqs.…”

Section: Nebular Excitation and Expansionmentioning

confidence: 99%

The evolution of planetary nebulae

Schönberner

Jacob

Sandín

et al. 2010

A&A

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Aims. By means of hydrodynamical models we do the first investigations of how the properties of planetary nebulae are affected by their metal content and what can be learned from spatially unresolved spectrograms of planetary nebulae in distant stellar systems. Methods. We computed a new series of 1D radiation-hydrodynamics planetary nebulae model sequences with central stars of 0.595 M surrounded by initial envelope structures that differ only by their metal content. At selected phases along the evolutionary path, the hydrodynamic terms were switched off, allowing the models to relax for fixed radial structure and radiation field into their equilibrium state with respect to energy and ionisation. The analyses of the line spectra emitted from both the dynamical and static models enabled us to systematically study the influence of hydrodynamics as a function of metallicity and evolution. We also recomputed selected sequences already used in previous publications, but now with different metal abundances. These sequences were used to study the expansion properties of planetary nebulae close to the bright cut-off of the planetary nebula luminosity function. Results. Our simulations show that the metal content strongly influences the expansion of planetary nebulae: the lower the metal content, the weaker the pressure of the stellar wind bubble, but the faster the expansion of the outer shell because of the higher electron temperature. This is in variance with the predictions of the interacting-stellar-winds model (or its variants) according to which only the central-star wind is thought to be responsible for driving the expansion of a planetary nebula. Metal-poor objects around slowly evolving central stars become very dilute and are prone to depart from thermal equilibrium because then adiabatic expansion contributes to gas cooling. We find indications that photoheating and line cooling are not fully balanced in the evolved planetary nebulae of the Galactic halo. Expansion rates based on widths of volume-integrated line profiles computed from our radiation-hydrodynamics models compare very well with observations of distant stellar system. Objects close to the bright cut-off of the planetary nebula luminosity function consist of rather massive central stars (>0.6 M ) with optically thick (or nearly thick) nebular shells. The halfwidth-half-maximum velocity during this bright phase is virtually independent of metallicity, as observed, but somewhat depends on the final AGB-wind parameters. Conclusions. The observed expansion properties of planetary nebulae in distant stellar systems with different metallicities are explained very well by our 1D radiation-hydrodynamics models. This result demonstrates convincingly that the formation and acceleration of a planetary nebula occurs mainly because of ionisation and heating of the circumstellar matter by the stellar radiation field, and that the pressure exerted by the shocked stellar wind is less important. Determinations of nebular abundances by means of photoionisa...

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“…CLOUDY and other similar photoionisation codes have already been applied in the evolutionary modelling of PNe by a number of authors, among them Volk (1992), Stasińska (1989), Stasińska & Szczerba (2001) Dopita & Meatheringham (1990), Dopita et al (1992), Dopita & Sutherland (2000), Phillips (2000). However, in all those cases the treatment of the underlying stellar population and of the nebula expansion was very crude, compared to our method of Paper I.…”

Section: Incorporation Of Cloudymentioning

confidence: 99%

Evolution of planetary nebulae

Marigo¹,

Girardi

Weiß

et al. 2004

A&A

154

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Abstract.We investigate the bright cut-off of the [O ] λ5007 planetary nebula luminosity function (PNLF), that has been suggested as a powerful extragalactic distance indicator in virtue of its observed invariance against populations effects. Theoretical PNLFs are constructed via Monte-Carlo simulations of populations of PNe, whose individual properties are described with the aid of recent PN synthetic models (Marigo et al. 2001, A&A, 378, 958), coupled to a detailed photoionisation code (CLOUDY). The basic dependences of the cut-off magnitude M * are then discussed. We find that : (i) In galaxies with recent or ongoing star formation, the modelled PNLF present M * values between −4 and −5, depending on model details. These are very close to the observationally-calibrated value for the LMC. (ii) In these galaxies, the PNLF cut-off is produced by PNe with progenitor masses of about 2.5 M , while less massive stars give origin to fainter PNe. As a consequence M * is expected to depend strongly on the age of the last burst of star formation, dimming by as much as 5 mag as we go from young to 10-Gyr old populations. (iii) Rather than on the initial metallicity of a stellar population, M * depends on the actual [O/H] of the observed PNe, a quantity that may differ significantly from the initial value (due to dredge-up episodes), especially in young and intermediate-age PN populations. (iv) Also the transition time from the end of AGB to the PN phase, and the nuclear-burning properties (i.e. Hor He-burning) of the central stars introduce non-negligible effects on M * . The strongest indication derived from the present calculations is a serious difficulty to explain the age-invariance of the cut-off brightness over an extended interval, say from 1 to 13 Gyr, that observations of PNLFs in galaxies of late-to-early type seem to suggest. We discuss the implications of our findings, also in relation to other interpretative pictures proposed in the past literature.

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The evolutionary sequence of planetary nebulae

Cited by 81 publications

References 0 publications

PFP 1: A Large Planetary Nebula Caught in the First Stages of ISM Interaction

PFP 1: A Large Planetary Nebula Caught in the First Stages of ISM Interaction

The evolution of planetary nebulae

Evolution of planetary nebulae

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